An Etymological Dictionary of Astronomy and Astrophysics
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فرهنگ ریشه شناختی اخترشناسی-اخترفیزیک

M. Heydari-Malayeri    -    Paris Observatory

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Number of Results: 13048 Search : far
kiloparsec (kpc)
  کیلوپارسک   
kilopârsek (#)

Fr.: kiloparsec   

A unit of distance equal to 1,000 → parsec (pc)s, or 3,260 → light-years.

kilo-; → parsec.

kilowatt-hour (kWh)
  کیلووات-ساعت   
kilowatt-sâ'at (#)

Fr.: kilowatt-heure   

A unit of energy equivalent to one kilowatt (1 kW) of power expended for one hour (1 h) of time. The kilowatt-hour is not a standard unit in any formal system, but it is commonly used to measure the consumption of electrical energy. To convert to → joules, use: 1 kWh = 3.6 × 106 J = 3.6 × 1013ergs.

kilo-; → watt-hour.

kinematic
  جنبشی، جنبشیک   
jonbeši, jonbešk

Fr.: cinématique   

Of or relating to → kinematics. Same as kinematical.

kinematics.

kinematic bias
  ورک ِ جنبشی   
varak-e jonbeši

Fr.: biais cinématique   

A systematic error introduced in a sample of stellar → proper motion data by higher velocity stars that are easier to measure.

kinematic; → bias.

kinematic viscosity
  وشکسانی ِ جنبشیک   
vošksâni-ye jonbešik

Fr.: viscosité cinématique   

The ratio of the → dynamic viscosity (η) to the density (ρ) of a fluid: ν = η/ρ. The unit of kinematic viscosity in the → SI system is m2s-1. In the → cgs system, cm2s-1, equal to 10-4 m2s-1, is called the → stokes (st).

kinematic; → viscosity.

kinematical
  جنبشی، جنبشیک   
jonbeši, jonbešik

Fr.: cinématique   

Of or relating to → kinematics. → kinematic.

kinematic; → -al.

kinematically decoupled core (KDC)
  مغزه‌ی ِ جنبشیکانه واجفسریده   
maqze-ye jonbešikâné vâjafsaridé

Fr.: cœur cinématiquement découplé   

A central, tightly bound stellar subsystem observed in some elliptical galaxies which rotates in the opposite direction with respect to the main body of the → elliptical galaxy. Elliptical galaxies are thought to be the result of the → merger of two or more sizable galaxies. A plausible scenario for how counter-rotating cores could form in such a merger is as follows. If at least one of the galaxies has a core region that is fairly tightly bound by the galaxy's gravity, and the direction in which the two galaxies orbit each other before merging is opposite to the direction of rotation of stars in that tightly bound core, it is likely that, after the merger, the tightly bound core will end up as the core of the new, larger galaxy, while retaining its original sense of rotation. The surrounding stars, on the other hand, will rotate in a different way dictated by the orbital motion of the galaxies around each other, before the merger. While this is a plausible scenario, it can only explain some of the counter-rotating cores. Recently A. Tsatsi et al. (2015, ApJ 802, L3) have shown that although the two → progenitor galaxies are initially following a → prograde orbit, strong reactive forces during the merger can cause a short-lived change of their orbital spin; the two progenitors follow a → retrograde orbit right before their final coalescence. This results in a central kinematic decoupling and the formation of a large-scale (~2 kpc radius) counter-rotating core at the center of the final elliptical-like merger remnant, while its outer parts keep the rotation direction of the initial orbital spin.

kinematical; → decouple; → core.

kinematics
  جنبشیک   
jonbešik

Fr.: cinématique   

The branch of mechanics dealing with the description of the motion of bodies or fluids without reference to the forces producing the motion.

From Gk. kinetikos "moving, putting in motion," from kinetos "moved," verbal adj. of kinein "to move;" PIE base *kei- "to move to and fro" (cf. Mod.Pers. šodan, šow- "to go; to become;" Av. šiyav-, š(ii)auu- "to move, go," šiyavati "goes," šyaoθna- "activity; action; doing, working;" O.Pers. šiyav- "to go forth, set," ašiyavam "I set forth;" Skt. cyu- "to move to and fro, shake about; to stir," cyávate "stirs himself, goes;" Goth. haitan "call, be called;" O.E. hatan "command, call").

Jonbešik, from jonbeš "motion" + -ik-ics. The first element from Mid.Pers. jumbidan, jumb- "to move," Lori, Laki jem "motion," related to gâm "step, pace;" O.Pers. gam- "to come; to go," Av. gam- "to come; to go," jamaiti "goes," gāman- "step, pace" (Mod.Pers. âmadan "to come"); Skt. gamati "goes;" Gk. bainein "to go, walk, step," L. venire "to come;" Tocharian A käm- "to come;" O.H.G. queman "to come;" E. come; PIE root *gwem- "to go, come."

kinetic
  جنبشی   
jonbeši (#)

Fr.: cinétique   

Of or relating to motion; caused by motion; characterized by movement.

From Gk. kinetikos "moving, putting in motion," from kinein "to move," → kinematics.

Jonbeši, adj. of jonbeš, verbal noun of jonbidan, → move.

kinetic energy
  کاروژ ِ جنبشی   
kâruž-e jonbeši

Fr.: énergie cinétique   

The energy which a body possesses as a consequence of its motion, defined as one-half the product of its mass m and the square of its speed v, i.e. 1/2 mv2.

kinetic; → energy.

kinetic helicity
  پیچاری ِ جنبشی   
picari-ye jonbeši

Fr.: hélicité cinétique   

In fluid mechanics, a quantity that describes helical flow. It is defined by the integrated scalar product of the velocity field and the → vorticity: KK = ∫ dVu . ( x u). In the absence of magnetic field, this quantity is conserved by the → Euler equation. See also → magnetic helicity.

kinetic; → helicity.

kinetic potential
  توند ِ جنبشیک   
tavand-e jonbešik

Fr.: potentiel cinétique   

Same as → Lagrangian function.

kinetic; → potential.

kinetic temperature
  دمای ِ جنبشی   
damâ-ye jonbeši (#)

Fr.: température cinétique   

The temperature of a gas defined in terms of the average kinetic energy of its atoms or molecules.

kinetic; → temperature.

kinetic theory of gases
  نگره‌ی ِ جنبشی ِ گاز‌ها   
negare-ye jonbeši-ye gâzhâ (#)

Fr.: théorie cinétique des gaz   

A theory that explains macroscopic properties of gases, such as pressure, temperature, or volume, by considering their molecular composition and motion.

kinetic; → theory; → gas.

Kippenhahn diagram
  نمودار ِ کیپنهان   
nemudâr-e Kippenhahn

Fr.: diagrame de Kippenhahn   

A plot representing the evolution of the internal structure of a star as a function of time. The x-axis indicates the time, the y-axis the mass, and a color or shading specifies convective regions. A vertical line through the graph corresponds to a model at a particular time.

Named after Rudolf Kippenhahn (1926-), a German astrophysicist; → diagram

Kirchhoff's law
  قانون ِ کیرشهوف   
qânun-e Kirchhoff (#)

Fr.: loi de Kirchhoff   

The radiation law which states that at thermal equilibrium the ratio of the energy emitted by a body to the energy absorbed by it depends only on the temperature of the body.

Gustav Robert Kirchhoff (1824-1887), a German physicist who made major contributions to the understanding of electric circuits, spectroscopy, and the emission of black-body radiation from heated objects; → law.

Kirkwood gaps
  گاف‌های ِ کرک‌وود   
gâfhâ-ye Kirkwood (#)

Fr.: lacunes de Kirkwood   

Regions in the asteroid belt within which few asteroids are found. The Kirkwood gaps are due to the perturbing effects of Jupiter through resonances with Jupiter's orbital period.

Named for the American astronomer Daniel Kirkwood (1814-1895), who Discovered them in 1866; → gap.

Kiso 5639
  کیسو ۵۶۳۹   
Kiso 5639

Fr.: Kiso 5639   

A → dwarf galaxy with a → kiloparsec size → starburst at one end, giving the system a → tadpole or → cometary shape. Also called LEDA-36252, KUG 1138+327. Its distance is 24.5 → megaparsecs (Mpc). The rotation speed of ~ 35 km s-1 combined with a radius of 1.2 kpc in the bright part of the disk implies that the corresponding → dynamical mass is 3 × 108/ sin2i Msun. This estimate is a factor of ~ 6 larger than the → stellar mass of 5 × 107 Msun from the → Sloan Digital Sky Survey photometry, but is comparable to the total → neutral hydrogen (H I) mass of ~ 3 × 108 Msun. The metallicity in the → starburst "head" appears to be less than in the rest of the galaxy (the "tail"). This peculiar pattern of metallicity, seen also in several other comparable galaxies, suggests that the starbursts in these systems were triggered by accreting a gas with lower metallicity than in the rest of the galaxy. The → Hubble Space Telescope observations of Kiso 5639 in six UV-optical and Hα filters were used to resolve the head and derive the star formation properties. The head contains 14 young → star clusters more massive than 104Msun and an overall clustering fraction for star formation of 25-40%. The Hα luminosity of the core region of the head is 8.8 ± 0.16 × 1039 erg s-1 inside an area of 3.6 × 3.6 square arcsec. The corresponding → star formation rate is ~ 0.04 Msun yr-1 (Elmegreen et al., 2018, arxiv/1805.08253, and references).

Kiso Survey of UV Bright Galaxies (Miyauchi-Isobe et al., 2010, Pub.Nat.Astro.Ob.Japan, 13, 9).

kite
  زغن   
zaqan (#)

Fr.: milan   

Any of several small birds of the hawk family Accipitridae that have long, pointed wings, feed on insects, carrion, reptiles, rodents, and birds, and are noted for their graceful, gliding flight (Dictionary.com).

M.E. kyte, O.E. cyta, cognate with Ger. Kauz "owl."

Zaqan "kite," of uknown origin.

Kleinmann-Law nebula
  میغ ِ کلاینمن-لاؤ   
miq-e Kainman-Law

Fr.: nébuleuse de Kleinmann-Law   

An strong, extended infrared source in the Orion Nebula, about 1 arcminute NW of the Trapezium and about 12 arcseconds south of the → Becklin-Neugebauer object. It dominates the infrared emission at wavelengths above 20 microns. It probably represents a cluster of young and forming stars embedded in a dusty molecular cloud.

Named after Douglas E. Kleinmann (1942-) and Frank J. Low (1933-), who first studied this object in 1967; → nebula.

<< < -es -iv -ti 21 a p abe abs abs aca acc acc acr act ada adh Adr aer AGB air Alf Alg all alp alt AM amo ana And ang ani ano Ant Ant apa apo app app Ara Arc ari Arr ash ass ast ast asy atm ato att aut ave axi Bab bal Bal bar bar bea Bek Bes bia Big bin bin bip biv bla bli blu Boh Bol Bos bou bra bri bro buo cal cal can cap car Car cat cat CCD Cen cen CH cha cha che Che chr cir cir cit cla clo clo clu Coa coe coh col col col com com com com com com com com Com con con con con con con con con con con con con Cop Cor cor cor cos cos cou cou Cow cre cri cro cry cur cya Cyg dan dar dat de- deb dec dec ded def deg del dem den dep des det dev dia dif dif dih dio Dir dis dis dis dis dis dis DO don dou dow dro dur dwa dyn Dys ear ebb ecl edg egg Ein Ela ele ele ele ele ell eme emp enc eng ent epi equ equ equ esc eth Eur Eve exa exc exe exi exp exp ext ext ext fac fal far fed Fer fer fie fin fir fis fla flo flu fol for for fou fra fre Fre fro fut G-t gal gal gam gas Gau Gem gen geo geo geo gia Gli Gol gra gra gra gra gre gri gui H I Hag hal har hat He- hea hel Hel her Hes hie hig his hom hor hot Hub Hug hur hyd hyd hyg hyp ice ide ima Ima imp imp inc inc ind ine inf inf inf ing inn ins ins int int int int int int int int inv Io ion iro isl iso iso Jac jet jud jur Kel Kep kil Klo Kui Lag lam Lap Lar lat law lea len lep Lib lig lim lin lin Lio lit loc LOF lon Lor low lum lun Lup Lyo mac mag mag mag mag mag mai man Mar mas mas mat Max mea mec Meg Mer Mer met met Met mic Mid Mil min Mir mit mod mod mol mon Mor mou mul mul mys nan Nat nau nec neo neu nev New NGC no nom non non nor not nuc nuc num nut obj obs obs occ ocu oft ome Oor ope opp opt opt orb ord ori ort osc out ove oxi pai pan par par par par pas pea pen per per per per Per per pha phi pho pho pho phy pio Pla pla pla pla Pla plu Poi pol pol pol poo pos pos pot pra pre pre pre pre pri pri pro pro pro pro pro Pro pro pse pul pur qua qua qua qua que rac rad rad rad rad rad rad ran rar ray rea rea rec rec red red ref ref reg rel rel rel ren res res res res ret rev Ric rig rin roc roo rot rot Rus Sac sal sat sca sca Sch sci Scu sec sec Sed sel Sel sen ser Sex Sha she sho sid sig sil sim sin siz sla Sma sno sof sol sol sol sol sou sou spa spa spe spe spe sph spi spi spr squ sta sta sta sta ste ste ste Sto Str str str sub sub suc sun sup sup sup sup sur swa syn syn tab tar tek tem ter tes the the the the Tho thr tid tim Tis Too Tor tra tra Tra tra tra tri tri tru Tul tur two Typ ult un- und uni uni unk upp Urc utt val var vec vel ver vib vio vir vis voi vor wan wat wav wax wea Wei whi Wil win WN9 wor X-r yel you zer zod > >>